The Energy Sources, the Physical Properties, and the Mass-loss History of SN 2017dio

Abstract

We study the energy sources, the physical properties of the ejecta and the circumstellar medium (CSM), as well as the mass-loss history of the progenitor of SN 2017dio which is a broad-lined Ic (Ic-BL) supernova (SN) having unusual light curves (LCs) and signatures of hydrogen-rich CSM in its early spectrum. We find that the temperature of SN 2017dio began to increase linearly about 20 days after the explosion. We use the ${}^{56}$Ni plus the ejecta-CSM interaction (CSI) model to fit the LCs of SN 2017dio, finding that the masses of the ejecta, the ${}^{56}$Ni, and the CSM are $\sim$ 12.41 M${}_{\odot }$, $\sim$ 0.17 M${}_{\odot }$, and $\sim$ 5.82 M${}_{\odot }$, respectively. The early-time photosphere velocity and the kinetic energy of the SN are respectively {$\sim$ 1.89 $\times 10^4$ km s${}^{-1}$} and $\sim$ 2.66 $\times 10^{52}$ erg, which are respectively comparable to those of SNe Ic-BL and hypernovae (HNe). We suggest that the CSM of SN 2017dio might be {from an luminous-blue-variable-like outburst or} pulsational pair instability $\sim$ 1.2$-$11.4 yr prior to the SN explosion{, or binary mass transfer}. {Moreover,} we find that its ejecta mass is larger than those of many SNe Ic-BL, and that its ${}^{56}$Ni mass ($M_{\mathrm{Ni}}$) is approximately equal to the mean (or median) value of $M_{\mathrm{Ni}}$ of SNe Ic-BL in the literature, but lower than $M_{\mathrm{Ni}}$ of prototype HNe (e.g., SN 1998bw and SN 2003dh).

Accepted for publication in ApJ, 17 pages, 4 figures, 3 tables